白光成像、行星际闪烁(IPS)、法拉第旋转是内日球层的主要遥感探测手段。白光成像能连续跟踪日冕物质抛射(CME)的传播和演化。遥感信号涉及视线方向的积分效应，具体是白光的汤姆逊散射效应和IPS的薄相屏近似等。遥感信号的反演和推断存在不确定性，需要CME运动学模型才能解读STEREO/HI所拍摄的CME白光影像和低频射电望远镜所记录的闪烁信号。本项目采用内日球层MHD数值模式正演和白光射电遥感观测反演，将模型计算结果与典型观测事件比对，研究行星际CME运动学和动力学，建立行星际CME动力学和白光射电观测表现的对应关系，加深理解遥感成像技术的探测能力，为空间天气预报发展策略和方法，利用观测数据检验MHD数值模式的正确性。基于该正演数值模式，预测行星际白光和射电的联合成像对CME的观测结果，预测将来部署在L4/L5点和太阳极轨的科学卫星所能拍摄的CME白光影像。

Observations in white light, interplanetary scintillation (IPS), and Faraday rotation are the main remote-sensing means for monitoring the inner heliosphere. Using white light imaging, interplanetary coronal mass ejections (CMEs) can be continuously tracked. Remote sensing signatures as a result of line-of-sight integration involve Thomson scattering effect for white light imaging and thin-phase-screen approximation for IPS signatures. Inversion and interpretation of remote sensing observation data suffer from large uncertainties, particularly at large elongations from the Sun. Kinematic CME models are needed to interpret brightness patterns of CMEs imaged by the STEREO/HIs, and low-frequency IPS signatures recorded by radio telescope array. In this proposal, we plan to use forward magnetohydrodynamic (MHD) modelling of the inner heliosphere in generating synthetic observations, analyze the observation data of STEREO/HI and IPS to infer local physical parameters, and compare modelling results with realistic observation events. We aim to uncover the kinematics and dynamics of interplanetary CMEs, establish the causal correspondence between CME dynamics and remotely observable signatures, understand remote-sensing capabilities of white-light and low-frequency radio techniques, and propose the feasible strategies and methods for space weather predicting. Our numerical MHD model is expected to be validated by observation data. Using our MHD model, we intend to predict the coordinated imaging observations of CMEs in white-light and radio, predict the white-light patterns of CMEs imaged by future satellites from the Lagrangian point L4/L5 and the solar polar orbit.